[1] A compiled empirical global Joule heating (CEJH) model is described in this study. This model can be used to study Joule heating patterns, Joule heating power, potential drop, and polar potential size in the high-latitude ionosphere and thermosphere, and their variations with solar wind conditions, geomagnetic activities, the solar EUV radiation, and the neutral wind. It is shown that the interplanetary magnetic field (IMF) orientation and its magnitude, the solar wind speed, AL index, geomagnetic K p index, and solar radio flux F 10.7 index are important parameters that control Joule heating patterns, Joule heating power, potential drop, and polar potential size. Other parameters, such as the solar wind number density (N sw ) and Earth's dipole tilt, do not significantly affect these quantities. It is also shown that the neutral wind can increase or reduce the Joule heating production, and its effectiveness mainly depends on the IMF orientation and its magnitude, the solar wind speed, AL index, K p index, and F 10.7 index. Our results indicate that for less disturbed solar wind conditions, the increase or reduction of the neutral wind contribution to the Joule heating is not significant compared to the convection Joule heating, whereas under extreme solar wind conditions, the neutral wind can significantly contribute to the Joule heating. Application of the CEJH model to the 16 July 2000 storm implies that the model outputs are basically consistent with the results from the AMIE mapping procedure. The CEJH model can be used to examine large-scale energy deposition during disturbed solar wind conditions and to study the dependence of the hemispheric Joule heating on the level of geomagnetic activities and the intensity of solar EUV radiation. This investigation enables us to predict global Joule heating patterns for other models in the high-latitude ionosphere and thermosphere in the sense of space weather forecasting.

Electron fluxes in the outer radiation belt are essentially governed by the dynamics of trapped particle motion in the inner magnetosphere, wherein the energetic particles execute complex periodic motions. Each motion is associated with one adiabatic invariant, namely, gyromotion around the magnetic field line, which is described as the first adiabatic invariant, bounce motion along the magnetic field line being identified as the second adiabatic invariant, and drift motion around the Earth as the third adiabatic invariant (Northrop & Teller, 1960; Roederer, 1970). Early spacecraft data revealed that phase space densities across the belts can vary significantly with time (see Roederer 1968), in which the violation of one or more adiabatic invariants can be required. This violation can occur due to the presence of several electrodynamic and magnetohydrodynamic processes in the magnetosphere, causing variations in the outer radiation belt electron flux, such as dropouts (e.g.,

Ion equatorial flux distributions, inverted from energetic neutral atom (ENA) images in different energy channels obtained by the HENA imager on the IMAGE satellite, are used to deduce the plasma ion temperature in the ring current. During the early period of the recovery phase of the strong storm on 12 August 2000, the deduced ion temperatures of the ring current are consistent with the values inferred from in situ LANL MPA measurements. The ion temperatures show a peak in the post‐midnight/pre‐dawn sector coincident with the peak in the equatorial ion distributions. The temperature, however, is more symmetrical than the ion flux implying that, at least in this part of the energy spectrum, the density variations make the major contribution to pressure gradients.